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Stochastic Starformation and Bubbles in the Large Magellanic Cloud

Published online by Cambridge University Press:  04 August 2017

J. V. Feitzinger
J. V. Feitzinger*
Affiliation:
Astronomisches Institut der Ruhr-Universität, Bochum, BRD

Extract

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Nearly all places in the LMC where ring nebulae or shell structures in the neutral or ionized interstellar medium are observed, an OB association and/or WR-stars can be located (Braunsfurth, Feitzinger, 1983). Several mechanisms have been propsoed to generate shell or bubble structures: stellar winds, supernovae explosions, evolving HII regions, sequential starformation, collapsing hydrogen clouds interacting with stellar winds and radiation pressure. Ordered motions resulting in a shell or bubble structure are the result of almost any point like energy injection into the interstellar medium. Therefore all the mechanisms result in similar morphological structures, thus similar shapes can have heterogeneous origins.

Type
Evolution
Information
Symposium - International Astronomical Union , Volume 108: Structure and Evolution of the Magellanic Clouds , 1984 , pp. 89 - 90
Copyright
Copyright © Reidel 1984 

References

Braunsfurth, E., Feitzinger, J.V., 1983, Astron. Astrophys., in press Google Scholar
Feitzinger, J.V., Glassgold, A.F., Gerola, H., Seiden, P., 1981, Astron. Astrophys. 98, 371 Google Scholar
Meaburn, J., 1980, Mon. Not. Roy. astr. Soc., 192, 365 CrossRefGoogle Scholar